Spectroscopic identification of r-process nucleosynthesis in a double neutron-star merger.

The merger of two neutron stars is predicted to give rise to three major detectable phenomena: a short burst of γ-rays, a gravitational-wave signal, and a transient optical-near-infrared source powered by the synthesis of large amounts of very heavy elements via rapid neutron capture (the r-process). Such transients, named 'macronovae' or 'kilonovae', are believed to be centres of production of rare elements such as gold and platinum. The most compelling evidence so far for a kilonova was a very faint near-infrared rebrightening in the afterglow of a short γ-ray burst at redshift z = 0.356, although findings indicating bluer events have been reported. Here we report the spectral identification and describe the physical properties of a bright kilonova associated with the gravitational-wave source GW170817 and γ-ray burst GRB 170817A associated with a galaxy at a distance of 40 megaparsecs from Earth. Using a series of spectra from ground-based observatories covering the wavelength range from the ultraviolet to the near-infrared, we find that the kilonova is characterized by rapidly expanding ejecta with spectral features similar to those predicted by current models. The ejecta is optically thick early on, with a velocity of about 0.2 times light speed, and reaches a radius of about 50 astronomical units in only 1.5 days. As the ejecta expands, broad absorption-like lines appear on the spectral continuum, indicating atomic species produced by nucleosynthesis that occurs in the post-merger fast-moving dynamical ejecta and in two slower (0.05 times light speed) wind regions. Comparison with spectral models suggests that the merger ejected 0.03 to 0.05 solar masses of material, including high-opacity lanthanides.

Highly polarized light from stable ordered magnetic fields in GRB 120308A.

After the initial burst of γ-rays that defines a γ-ray burst (GRB), expanding ejecta collide with the circumburst medium and begin to decelerate at the onset of the afterglow, during which a forward shock travels outwards and a reverse shock propagates backwards into the oncoming collimated flow, or 'jet'. Light from the reverse shock should be highly polarized if the jet's magnetic field is globally ordered and advected from the central engine, with a position angle that is predicted to remain stable in magnetized baryonic jet models or vary randomly with time if the field is produced locally by plasma or magnetohydrodynamic instabilities. Degrees of linear polarization of P ≈ 10 per cent in the optical band have previously been detected in the early afterglow, but the lack of temporal measurements prevented definitive tests of competing jet models. Hours to days after the γ-ray burst, polarization levels are low (P < 4 per cent), when emission from the shocked ambient medium dominates. Here we report the detection of P =28(+4)(-4) per cent in the immediate afterglow of Swift γ-ray burst GRB 120308A, four minutes after its discovery in the γ-ray band, decreasing to P = 16(+5)(-4) per cent over the subsequent ten minutes. The polarization position angle remains stable, changing by no more than 15 degrees over this time, with a possible trend suggesting gradual rotation and ruling out plasma or magnetohydrodynamic instabilities. Instead, the polarization properties show that GRBs contain magnetized baryonic jets with large-scale uniform fields that can survive long after the initial explosion.

The unusual gamma-ray burst GRB 101225A explained as a minor body falling onto a neutron star.

The tidal disruption of a solar-mass star around a supermassive black hole has been extensively studied analytically and numerically. In these events, the star develops into an elongated banana-shaped structure. After completing an eccentric orbit, the bound debris falls into the black hole, forming an accretion disk and emitting radiation. The same process may occur on planetary scales if a minor body passes too close to its star. In the Solar System, comets fall directly into our Sun or onto planets. If the star is a compact object, the minor body can become tidally disrupted. Indeed, one of the first mechanisms invoked to produce strong gamma-ray emission involved accretion of comets onto neutron stars in our Galaxy. Here we report that the peculiarities of the 'Christmas' gamma-ray burst (GRB 101225A) can be explained by a tidal disruption event of a minor body around an isolated Galactic neutron star. This would indicate either that minor bodies can be captured by compact stellar remnants more frequently than occurs in the Solar System or that minor-body formation is relatively easy around millisecond radio pulsars. A peculiar supernova associated with a gamma-ray burst provides an alternative explanation.

Broadband observations of the naked-eye gamma-ray burst GRB 080319B.

Long-duration gamma-ray bursts (GRBs) release copious amounts of energy across the entire electromagnetic spectrum, and so provide a window into the process of black hole formation from the collapse of massive stars. Previous early optical observations of even the most exceptional GRBs (990123 and 030329) lacked both the temporal resolution to probe the optical flash in detail and the accuracy needed to trace the transition from the prompt emission within the outflow to external shocks caused by interaction with the progenitor environment. Here we report observations of the extraordinarily bright prompt optical and gamma-ray emission of GRB 080319B that provide diagnostics within seconds of its formation, followed by broadband observations of the afterglow decay that continued for weeks. We show that the prompt emission stems from a single physical region, implying an extremely relativistic outflow that propagates within the narrow inner core of a two-component jet.

An origin for short gamma-ray bursts unassociated with current star formation.

Two short (< 2 s) gamma-ray bursts (GRBs) have recently been localized and fading afterglow counterparts detected. The combination of these two results left unclear the nature of the host galaxies of the bursts, because one was a star-forming dwarf, while the other was probably an elliptical galaxy. Here we report the X-ray localization of a short burst (GRB 050724) with unusual gamma-ray and X-ray properties. The X-ray afterglow lies off the centre of an elliptical galaxy at a redshift of z = 0.258 (ref. 5), coincident with the position determined by ground-based optical and radio observations. The low level of star formation typical for elliptical galaxies makes it unlikely that the burst originated in a supernova explosion. A supernova origin was also ruled out for GRB 050709 (refs 3, 31), even though that burst took place in a galaxy with current star formation. The isotropic energy for the short bursts is 2-3 orders of magnitude lower than that for the long bursts. Our results therefore suggest that an alternative source of bursts--the coalescence of binary systems of neutron stars or a neutron star-black hole pair--are the progenitors of short bursts.

Interchangeability of phosphorylation coupling factors in photosynthetic and respiratory energy conversion.

The nonsulfur purple photosynthetic bacterium Rhodopseudomonas capsulata can obtain energy for growth either by anaerobic photophosphorylation or dark oxidative (aerobic) phosphorylation. Successful resolution of phosphorylation coupling factors from energy-converting membranes of this bacterium permitted tests for reciprocal function of such protein factors in oxidative-and photophosphorylation processes. Evidence was obtained for the interchangeability of coupling factor preparations from dark-grown and photosynthetically grown cells in both kinds of energy conversion.

Compact radio emission indicates a structured jet was produced by a binary neutron star merger.

The binary neutron star merger event GW170817 was detected through both electromagnetic radiation and gravitational waves. Its afterglow emission may have been produced by either a narrow relativistic jet or an isotropic outflow. High-spatial-resolution measurements of the source size and displacement can discriminate between these scenarios. We present very-long-baseline interferometry observations, performed 207.4 days after the merger by using a global network of 32 radio telescopes. The apparent source size is constrained to be smaller than 2.5 milli-arc seconds at the 90% confidence level. This excludes the isotropic outflow scenario, which would have produced a larger apparent size, indicating that GW170817 produced a structured relativistic jet. Our rate calculations show that at least 10% of neutron star mergers produce such a jet.

Swift and NuSTAR observations of GW170817: Detection of a blue kilonova.

With the first direct detection of merging black holes in 2015, the era of gravitational wave (GW) astrophysics began. A complete picture of compact object mergers, however, requires the detection of an electromagnetic (EM) counterpart. We report ultraviolet (UV) and x-ray observations by Swift and the Nuclear Spectroscopic Telescope Array of the EM counterpart of the binary neutron star merger GW170817. The bright, rapidly fading UV emission indicates a high mass (≈0.03 solar masses) wind-driven outflow with moderate electron fraction (Ye ≈ 0.27). Combined with the x-ray limits, we favor an observer viewing angle of ≈30° away from the orbital rotation axis, which avoids both obscuration from the heaviest elements in the orbital plane and a direct view of any ultrarelativistic, highly collimated ejecta (a γ-ray burst afterglow).

Energy transduction in photosynthetic bacteria. VIII. Activation of the energy-transducing ATPase by inorganic phosphate.

ATPase activity and ATP-induced energization of photosynthetic membranes from Rhodopseudomonas capsulata are stimulated by phosphate; the maximum stimulatory effect occurs at a concentration between 1 and 2 mM. The sensitivity of the ATPase to oligomycin increases in the presence of phosphate since all the Pi-stimulated activity is inhibited by this antibiotic. Aurovertin, which has no effect on ATPase in the absence of phosphate, inhibits completely the activity elicited by this anion. The addition of Pi induces a substantial increase in the V of ATPase activity without changing the affinity of the enzyme for ATP or ADP. Arsenate, at the same concentrations, produces effects very similar to those of phosphate. The stimulation by arsenate of the transfer of energy from ATP to the membrane suggests a non-hydrolytic role of this anion as a modifier of the ATPase activity.

Energy transduction in photosynthetic bacteria. VII. Inhibition of the coupling ATPase by N-ethylmaleimide related to the energized state of the membrane.

N-Ethylmaleimide, at millimolar concentrations, irreversibily inhibits photophosphorylation and ATPase activity of photosynthetic membranes from Rhodopseudomonas capsulata. The inhibitory effect of N-ethylmaleimide is evident only the membranes are preincubated with the inhibitor in the light and in the absence of phosphorylation substrates. ADP and orthophosphate (or arsenate) exert a protective effect against the inhibition if they are present during the preillumination stage. The energization of the membrane by ATP hydrolysis, measured as ATP-induced quenching of 9-aminoacridine fluorescence, also is inhibited irreversibly by N-ethylmaleimide. Uncouplers protect the ATPase from inhibition by N-ethylmaleimide at concentrations at which they inhibit photophosphorylation. The ATPase, as measured either in the dark or in the light, is also inhibited by carbonylcyanide p-trifluoromethoxypenylhydrazone in parallel with photophosphorylation. These results are interpreted as evidence that the high-energy state of the membrane induces a conformational change of the ATPase, making it sensitive to attack by N-ethylmaleimide; this conformational change might be related to the active state of the ATPase.

Energy tranduction in photosynthetic bacteria. XI. Further resolution of cytochromes of b type and the nature of the co-sensitive oxidase present in the respiratory chain of Rhodopseudomonas capsulata.

1. In membranes prepared from dark grown cells of Rhodopseudomonas capsulata, five cytochromes of b type (E'0 at pH 7.0 +413+/-5, +270+/-5, +148+/-5, +56+/-5 and -32+/-5 mV) can be detected by redox titrations at different pH values. The midpoint potentials of only three of these cytochromes (b148, b56, and b-32) vary as a function of pH with a slope of 30 mV per pH unit. 2. In the presence of a CO/N2 mixture, the apparent E'0 of cytochrome b270 shifts markedly towards higher potentials (+355mV); a similar but less pronounced shift is apparent also for cytochrome b150. The effect of CO on the midpoint potential of cytochrome b270 is absent in the respiration deficient mutant M6 which possesses a specific lesion in the CO-sensitive segment of the branched respiratory chain present in the wild type strain. 3. Preparations of spheroplasts with lysozyme digestion lead to the release of a large amount of cytochrome c2 and of virtually all cytochrome cc'. These preparations show a respiratory chain impaired in the electron pathway sensitive to low KCN concentration, in agreement with the proposed role of cytochrome c2 in this branch; on the contrary, the activity of the CO-sensitive branch remains unaffected, indicating that neither cytochrome c2 nor the CO-binding cytochrome cc' are involved in this pathway. 4. Membranes prepared from spheroplasts still possess a CO-binding pigment characterized by maxima at 420.5, 543 and 574 nm and minima at 431, 560 nm in C0-difference spectra and with an alpha band at 562.5 nm in reduced minus oxidized difference spectra. This membrane-bound cytochrome, which is coincident with cytochrome b270, can be classified as a typical cytochrome "0" and considered the alternative CO-sensitive oxidase.

Energy transduction in photosynthetic bacteria. X. Composition and function of the branched oxidase system in wild type and respiration deficient mutants of Rhodopseudomonas capsulata.

The respiratory chain of Rhodopseudomonas capsulata, strain St. Louis and of two respiration deficient mutants (M6 and M7) has been investigated by examining the redox and spectral characteristics of the cytochromes and their response to substrates and to specific respiratory inhibitors. Since the specific lesions of M6 and M7 have been localized on two different branches of the multiple oxidase system of the wild type strain, the capability for aerobic growth of these mutants can be considered as a proof of the physiological significance of both branched systems "in vivo". Using M6 and M7 mutants the response of the branched chain to respiratory inhibitors could be established. Cytochrome oxidase activity, a specific function of an high potential cytochrome b (E'0 = +413 mV) is sensitive to low concentrations of KCN (5-10(-5) M); CO is a specific inhibitor of an alternative oxidase, which is also inhibited by high concentrations of KCN (10(-3) M). Antimycin A inhibits preferentially the branch of the chain affected by low concentrations of cyanide. Redox titrations and spectral data indicate the presence in the membrane of three cytochromes of b type (E'0 = +413, +260, +47 vM) and two cytochromes of c type (E'0 = +342, +94 mV). A clear indication of the involvement in respiration of cytochrome b413, cytochrome c342 and cytochrome b47 has been obtained. Only 50% of the dithionite reducible cytochrome b can be reduced by respiratory substrates also in the presence of high concentrations of KCN or in anaerobiosis. The presence and function of quinones in the respiratory electron transport system has been clearly demonstrated. Quinones, which are reducible by NADH and succinate to about the same extent can be reoxidized through both branches of the respiratory chain, as shown by the response of their redox state to KCN. The possible site of the branching of the electron transport chain has been investigated comparing the per cent level of reduction of quinones and of cytochromes b and c as a function of KCN concentrations in membranes from wild type and M6 mutants cells. The site of the branching has been localized at the level of quinones-cytochrome b47. A tentative scheme of the respiratory chains operating in Rhodopseudomonas capsulata, St. Louis and in the two respiration deficient mutants, M6 and M7 is presented.

The induction kinetics of bacterial photophosphorylation. Threshold effects by the phosphate potential and correlation with the amplitude of the carotenoid absorption band shift.

1. ATP synthesis (monitored by luciferin-luciferase) can be elicited by a single turnover flash of saturating intensity in chromatophores from Rhodopseudomonas capsulata, Kb1. The ATP yield from the first to the fourth turnover is strongly influenced by the phosphate potential: at high phosphate potential (-11.5 kcal/mol) no ATP is formed in the first three turnovers while at lower phosphate potential (-8.2 kcal/mol) and the yield in the first flash is already one half of the maximum, which is reached after 2-3 turnovers. 2. The response to ionophores indicates that the driving force for ATP synthesis in the first 20 turnovers is mainly given by a membrane potential. The amplitude of the carotenoid band shift shows that during a train of flashes an increasing delta psi is built up, which reaches a stationary level after a few turnovers; at high phosphate potential, therefore, more turnovers of the same photosynthetic unit are required to overcome an energetic threshold. 3. After several (six to seven) flashes the ATP yield becomes constant, independently from the phosphate potential; the yield varies, however, as a function of dark time (td) between flashes, with an optimum for td = 160-320 ms. 4. The decay kinetics of the high energy state generated by a long (125 ms) flash have been studied directly measuring the ATP yield produced in post-illumination by one single turnover flash, under conditions of phosphate potential (-10 kcal/mol), which will not allow ATP formation by one single turnover. The high energy state decays within 20 s after the illumination. The decay rate is strongly accelerated by 10(-8) M valinomycin. 5. Under all the experimental conditions described, the amplitude of the carotenoid signal correlates univocally with the ATP yield per flash, demonstrating that this signal monitores accurately an energetic state of the membrane directly involved in ATP synthesis. 6. Although values of the carotenoid signal much larger than the minimal threshold are present, relax slowly, and contribute to the energy input for phosphorylation, no ATP is formed unless electron flow is induced by a single turnover flash. 7. The conclusions drawn are independent from the assumption that a delta psi between bulk phases is evaluable from the carotenoid signal.

Photosynthetic control and estimation of the optimal ATP: electron stoichiometry during flash activation of chromatophores from Rhodopseudomonas capsulata.

(1) When chromatophores from Rhodopseudomonas capsulata Ala pho+ are exposed to a train of high-frequency, saturating flashes the kinetics of the reaction centre bacteriochlorophyll absorption change enter a pseudo steady-state in which the extent of oxidation during the flashes is equal to the extent of reduction in between the flashes. The level of the pseudo steady-state is lowered by the presence of a phosphate acceptor system, raised by further addition of oligomycin, lowered by a combination of nigericin and valinomycin and raised by antimycin A. (2) In the pseudo steady-state, the extent of reaction centre bacteriochlorophyll oxidation taking place during the flash may be estimated by subtraction from the total concentration of reaction centre bacteriochlorophyll. This value is equated with the amount of electrons transported through the photosynthetic chain. Comparison with the measured ATP yield per flash in the pseudo steady-state permits calculation of the ATP: two electron ratio. The value of the ratio is 1.1 for flash frequencies between 3 and 12.5 Hz and declines at lower and higher frequencies. The ATP: two electron ratio is approximately halved in the presence of antimycin A. (3) An alternative estimate of the ATP: two electron ratio, based on the assumption that high-frequency flashes approximate to the condition of continuous illumination, was approx. 0.8.

Asymmetry of an energy transducing membrane the location of cytochrome c2 in Rhodopseudomonas spheroides and Rhodopseudomonas capsulata.

Monospecific antibodies have been prepared against cytochrome c2 from Rhodopseudomonas spheroides and Rhodopseudomonas capsulata, and against cytochrome c' from Rps. capsulata. These antibodies precipitated their respective antigens, but did not cross react with a wide range of procaryotic or eucaryotic cytochromes, or with other bacterial proteins. The cytochromes produced during aerobic growth were immunologically indistinguishable from those produced during photosynthetic growth. Cytochrome c2 is located in vivo in the periplasmic space between the cell was and the cell membrane, and when chromatophores are prepared from whole cells the cytochrome becomes trapped inside these vesicles. The implications of these results to energy coupling in the photosynthetic bacteria are discussed.

GRB 130427A: a nearby ordinary monster.

Long-duration gamma-ray bursts (GRBs) are an extremely rare outcome of the collapse of massive stars and are typically found in the distant universe. Because of its intrinsic luminosity (L ~ 3 × 10(53) ergs per second) and its relative proximity (z = 0.34), GRB 130427A reached the highest fluence observed in the γ-ray band. Here, we present a comprehensive multiwavelength view of GRB 130427A with Swift, the 2-meter Liverpool and Faulkes telescopes, and by other ground-based facilities, highlighting the evolution of the burst emission from the prompt to the afterglow phase. The properties of GRB 130427A are similar to those of the most luminous, high-redshift GRBs, suggesting that a common central engine is responsible for producing GRBs in both the contemporary and the early universe and over the full range of GRB isotropic energies.